A Comparative Study of the Absolute Magnitude Distributions of Supernovae

Richardson, D.; Branch, David; Casebeer, D.; Millard, Jennifer; Thomas, Romain; Baron, E.

doi:10.1086/338318

Cited by 221 publications

(324 citation statements)

References 35 publications

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“…We note, however, that the uncertainty in the relative fractions within the corecollapse types is quite large. For instance, Smartt et al (2009) found a much higher fraction of type Ib/c (29%) than Richardson et al (2002), while their estimate of the number of type IIL is about a factor 10 lower than what has been assumed here. Clearly, significantly larger data-sets are needed to determine the CC rates accurately, both at low and high redshifts.…”

Section: Supernova Subtypescontrasting

confidence: 63%

Near-IR search for lensed supernovae behind galaxy clusters

Goobar

Paech

Stanishev³

et al. 2009

A&A

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Aims. Powerful gravitational telescopes in the form of massive galaxy clusters can be used to enhance the light collecting power over a limited field of view by about an order of magnitude in flux. This effect is exploited here to increase the depth of a survey for lensed supernovae at near-IR wavelengths. Methods. We present a pilot supernova search programme conducted with the ISAAC camera at VLT. Lensed galaxies behind the massive clusters A1689, A1835, and AC114 were observed for a total of 20 h divided into 2, 3, and 4 epochs respectively, separated by approximately one month to a limiting magnitude J < ∼ 24 (Vega). Image subtractions including another 20 h worth of archival ISAAC/VLT data were used to search for transients with lightcurve properties consistent with redshifted supernovae, both in the new and reference data. Results. The feasibility of finding lensed supernovae in our survey was investigated using synthetic lightcurves of supernovae and several models of the volumetric type Ia and core-collapse supernova rates as a function of redshift. We also estimate the number of supernova discoveries expected from the inferred star-formation rate in the observed galaxies. The methods consistently predict a Poisson mean value for the expected number of supernovae in the survey of between N SN = 0.8 and 1.6 for all supernova types, evenly distributed between core collapse and type Ia supernovae. One transient object was found behind A1689, 0.5 from a galaxy with photometric redshift z gal = 0.6 ± 0.15. The lightcurve and colors of the transient are consistent with being a reddened type IIP supernova at z SN = 0.59. The lensing model predicts 1.4 mag of magnification at the location of the transient, without which this object would not have been detected in the near-IR ground-based search described in this paper (unlensed magnitude J ∼ 25). We perform a feasibility study of the potential for lensed supernovae discoveries with larger and deeper surveys and conclude that the use of gravitational telescopes is a very exciting path for new discoveries. For example, a monthly rolling supernova search of a single very massive cluster with the HAWK-I camera at VLT would yield > ∼ 10 lensed supernova lightcurves per year, where type Ia supernovae would constitute about half of the expected sample. Conclusions.

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Section: Supernova Subtypescontrasting

confidence: 63%

Near-IR search for lensed supernovae behind galaxy clusters

Goobar

Paech

Stanishev³

et al. 2009

A&A

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“…This value corresponds roughly to the limiting magnitude of SN surveys, especially the LOSS SN Survey (van den Bergh et al 2005) providing a large 1 The R 25 radius is the radius of the 25 mag arcsec −2 B-band isophote. (and long-dashed) lines show the average magnitude (and its dispersion) given in Richardson et al (2002). Almost no SN are found in the shaded area (apparent magnitudes fainter than 19) because it corresponds roughly to the limiting magnitude of the sample (see text).…”

Section: The Supernova Samplementioning

confidence: 97%

Relative frequencies of supernovae types: dependence on host galaxy magnitude, galactocentric radius, and local metallicity

Boissier¹,

Prantzos²

2009

A&A

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Context. Stellar evolution theory suggests that the relationship between number ratios of supernova (SN) types and metallicity can provide important information about the physical properties of the progenitor stars (e.g., mass, metallicity, rotation, binarity). Aims. We investigate the metallicity dependence of the number ratios of various SN types, using a large sample of SN along with information about their radial position within, and magnitude of, their host galaxy. Methods. We derive global galaxy gas-phase metallicities (using the well-known metallicity-luminosity relation) and local metallicities, i.e., at the position of the SN. In the latter case, we use the empirical fact that the metallicity gradients in disk galaxies are ∼constant when expressed in dex/R 25 . Results. We confirm a dependence of the N(Ibc)/N(II) ratio on metallicity. Single star models with rotation and binary star models with no rotation appear to reproduce equally well the metallicity dependence. The size of our sample does not allow significant conclusions about the N(Ic)/N(Ib) ratio. Finally, we find an unexpected metallicity dependence of the ratio of thermonuclear to core collapse supernovae, which we interpret in terms of the star formation properties of the host galaxies.

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“…The most luminous SLSNe observed have M V ∼ −22.5 (Gal-Yam 2012). In contrast, regular supernovae typically peak in the range −17 < M V < −20 (Richardson et al 2002).…”

Section: Superluminous Supernovaementioning

confidence: 99%

Understanding extreme quasar optical variability with CRTS – I. Major AGN flares

Graham¹,

Djorgovski²,

Drake³

et al. 2017

Monthly Notices of the Royal Astronomical Society

120

133

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There is a large degree of variety in the optical variability of quasars and it is unclear whether this is all attributable to a single (set of) physical mechanism(s). We present the results of a systematic search for major flares in active galactic nucleus (AGN) in the Catalina Real-time Transient Survey as part of a broader study into extreme quasar variability. Such flares are defined in a quantitative manner as being atop of the normal, stochastic variability of quasars. We have identified 51 events from over 900 000 known quasars and high-probability quasar candidates, typically lasting 900 d and with a median peak amplitude of m = 1.25 mag. Characterizing the flare profile with a Weibull distribution, we find that nine of the sources are well described by a single-point single-lens model. This supports the proposal by Lawrence et al. that microlensing is a plausible physical mechanism for extreme variability. However, we attribute the majority of our events to explosive stellar-related activity in the accretion disc: superluminous supernovae, tidal disruption events and mergers of stellar mass black holes.

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A Comparative Study of the Absolute Magnitude Distributions of Supernovae

Cited by 221 publications

References 35 publications

Near-IR search for lensed supernovae behind galaxy clusters

Near-IR search for lensed supernovae behind galaxy clusters

Relative frequencies of supernovae types: dependence on host galaxy magnitude, galactocentric radius, and local metallicity

Understanding extreme quasar optical variability with CRTS – I. Major AGN flares

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